Equation of state for neutron stars: Hyperon mixing in SU(3) flavor symmetry

Using various kinds of relativistic mean-field models as well as the quark-meson coupling model, we study in detail the properties of neutron stars. We find that the equation of state in SU(3) flavor symmetry can support a neutron star with mass of $(1.8\sim 2.1)M_{\odot }$ even if hyperons exist inside the core of a neutron star.